The depth of the Ca ii K line is used in main sequence A-type stars as the prime estimator of
their effective temperature ([1]}). However, following other works
devoted to the determination of stellar parameters of HAeBes [2]}, [3]}, this line has also been excluded from the whole procedure devised in this work. The reason is that most stars in the sample show Ca ii K lines with circumstellar contributions and/or peculiar profiles that pure photospheric models are not able to reproduce. In addition, the blue part of the spectrum would be affected by veiling in those cases where the accretion contribution to the total flux starts to be comparable to the photospheric flux.
